New results for reaction rate of the proton radiative capture on 3 H

Dubovichenko, S. B.; Dzhazairov-Kakhramanov, A. V.; Afanasyeva, N.V.

doi:10.1016/j.nuclphysa.2017.04.006

Cited by 18 publications

(12 citation statements)

References 63 publications

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“…As seen from Table 1, this value is in a good agreement with results of works [43,44]. The linear extrapolation of data [43] in the form S(E) = 0.237E(MeV) + 0.40 (5) is shown in Figure 2 by the blue dashed line and leads to the results at zero energy of 0.40(1) keVb. This line describes data [48] shown in Figure 2 by circles at energies up to 2.5 MeV quite well.…”

Section: The Astrophysical S-factorsupporting

confidence: 86%

“…Furthermore, in [13,14] in the MPCM with tensor forces the possibility of the correct reproduction practically of all characteristics of 6 Li was demonstrated, including its quadrupole momentum. Subsequently, in [15][16][17][18] on the basis of the MPCM we have presented the possibility of description of the astrophysical S-factors or the total cross sections of almost 30 radiative capture processes, namely, p 2 H, n 2 H, p 3 H, p 6 Li, n 6 Li, p 7 Li, n 7 Li, p 9 Be, n 9 Be, p 10 B, n 10 B, p 11 B, n 11 B, p 12 C, n 12 C, p 13 C, n 13 C, p 14 C, n 14 C, n 14 N, p 15 N, n 15 N, n 16 O and 2 H 4 He, 3 He 4 He, 3 H 4 He, 4 He 12 C systems at thermal and astrophysical energies (see also [2][3][4][5][6][7]). Continuing study of thermonuclear reactions in the frame of the modified potential cluster model with forbidden states [15][16][17][18] let us consider the 16 O(p,) 17 F process, which takes part of the CNO cycle [15,16] and has additional interest, since it is the reaction at the last nucleus of 1p-shell with the forming of 17 F that get out its limit.…”

Section: Introductionmentioning

confidence: 99%

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New results for radiative proton capture on 16O at astrophysical energies

Dubovichenko¹,

Dzhazairov-Kakhramanov²

2018

Indian J Phys

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The possibility of description of the experimental data for the astrophysical S-factor of the proton radiative capture on 16 O to the ground and first excited states of 17 F was considered in the frame of the modified potential cluster model with forbidden states and classification of the states according to Young tableaux. It was shown that on the basis of the E1 transitions from the P states of p 16 O scattering to the bound states of 17 F in the p 16 O channel, it generally succeed to explain the value of measured astrophysical S-factors and reaction rates at astrophysical energies. The total cross sections, astrophysical S-factor from 10 keV and reaction rate at temperatures from 0.01 to 5 T9.

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Section: The Astrophysical S-factorsupporting

confidence: 86%

Section: Introductionmentioning

confidence: 99%

New results for radiative proton capture on 16O at astrophysical energies

Dubovichenko¹,

Dzhazairov-Kakhramanov²

2018

Indian J Phys

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“…For BS of nuclei formed as a result of capture reaction in cluster channel, which coincides with the initial particles, intercluster potentials are constructed based on the description of binding energy of these particles in final nucleus and some basic characteristics of such states (see, for example, Refs. [16][17][18]. Usually, these are charge radius and asymptotic constant (AC), meanwhile, the characteristics of clusters connected in nucleus are identified with characteristics of the correspondent free nuclei.…”

Section: Physical Aspects Of the Used Methodsmentioning

confidence: 99%

“…We use a simple Gaussian potential of the form as in our previous works Refs. 1,2,[16][17][18]22, for description partial intercluster interaction (in this case between a nucleon and a nucleus),…”

Section: Potentials Of the P 14 N Interaction In Different Statesmentioning

confidence: 99%

Reaction rate of p14N →15Oγ capture to all bound states in potential cluster model

Dubovichenko

Burkova

Dzhazairov-Kakhramanov

et al. 2020

Int. J. Mod. Phys. E

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Review of calculation results for astrophysical S-factor of the 14 N(р,  15 О capture reaction in the p 14 N channel of 15 O was presented. It was carried out in the frame of the modified potential cluster model, taking into account resonances in the 15 O spectrum up to 3.2 MeV at energy of incident protons varying from 30 keV to 5 MeV. It is possible to describe experimental data for the astrophysical Sfactors of the radiative proton capture on 14 N to five excited states of 15 O at excitation energies from 5.18 MeV to 6.86 MeV, only under assumption, that all five resonances are D scattering waves. Quality new physical interpretation of the capture mechanism is discussed in this channel to the ground state of 15 O. Carried out by us assumption that the ground state of 15 O is determined by the p 14 N * channel with excited 14 N * cluster, immediately allowed us to correctly describe order of values of the experimental S-factor for capture to this state. Taking into account these results, the total S-factor of the proton capture on 14 N and the reaction rates to the ground and five excited states of 15 O were determined at temperatures from 0.01 to 10 T 9 . The parametrization of the total reaction rate with a simple form is performed, which allows to obtain  2 equal to 0.06 with 5% errors of the calculated rate.1. With an excitation energy of 5.183(1) MeV above BS or -2.1141 MeV in c.m. Ref. 26 relative to threshold of the р 14 N channel, there is a first excited, but bound in this channel, state with the moment J  = 1/2 + , which can be matched to the doublet 2 S 1/2 wave with FS. Although such state can, of course, be considered as a quartet 4 D 1/2 wave with FS.2. The second ES (2 nd ES) with an excitation energy of 5.2409(3) MeV Ref. 26 relative to the GS or -2.0562 MeV relative to the threshold of the р 14 N channel has J  = 5/2 + and it can be matched to the mixture of doublet and quartet 2+4 D 5/2 waves with FS.3. The third excited state (3 rd ES) at an excitation energy of 6.1763(17) MeV Ref. 26 relative to the GS or -1.1208 MeV relative to channel threshold has J  = 3/2and it can be compared to a mixture of doublet and quartet 2+4 Р 3/2 -waves without an associated FS.4. The fourth excited state (4 th ES) has an excitation energy of 6.7931(17) MeV relative to the GS or -0.504 MeV Ref. 26 or relative to the channel threshold has J  = 3/2 + and it can be compared with the quartet 4 S 3/2 wave with the FS. Of course, this state may also be a mixture of doublet and quartet 2+4 D 3/2 waves with the FS.5. The fifth excited state (5 th ES) with an excitation energy of 6.8594(9) MeV Ref. 26 relative to the GS or -0.4377 MeV relative to the channel threshold has J  = 5/2 + and it can also be compared to a mixture of doublet and quartet 2+4 D 5/2 wave with the FS 6. There is another bound state in the р 14 N channel with J  = 7/2 + at an excitation energy of 7.2759(6) MeV Ref. 26 relative to the GS or -0.0212 MeV relative to the threshold of the considered channel, which can be compared to the 4 D 7/2 s...

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“…If both methods are used for the same system of particles, it is possible to control the correctness of the search for the binding energy and WF of the state. We already have used such an approach for p 2 H and p 3 H systems in [28,46] and demonstrated that the FDM provides more precise description of the systems. Below we present the FDM approach.…”

Section: Appendix Amentioning

confidence: 99%

The $^6$Li$(p, γ)^7$Be reaction rate in the light of the new LUNA data

Dubovichenko¹,

Tkachenko²,

Kezerashvili³

et al. 2022

Preprint

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We present new calculations of the astrophysical S −factor and reaction rate for the 6 Li(p,γ) 7 Be reaction at energies of 10 keV to 5 MeV in the framework of a modified potential cluster model with forbidden states, including low lying resonances. The astrophysical S (E)−factor is compared with the available experimental data and calculations done within different models. The results for the S −factor are in good agreement with the data set (for E < 0.3 MeV) and calculations (for E < 0.6 MeV) of LUNA collaboration (Phys. Rev. C 102, 052802, 2020). The recommended extrapolated zero value S (0) turned out to be 101 eV ⋅ b. Using the theoretical total cross-sections, the 6 Li(p,γ) 7 Be capture reaction rate is calculated at temperatures ranging from 0.01 to 10 T 9 and compared with NACRE and NACRE II. Analytical expressions for the S −factor and reaction rate are given, and the effect of low-lying resonances on the reaction rate is estimated. We suggest to update the NACRE and NACRE II databases in light of the new LUNA data and present calculations.

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New results for reaction rate of the proton radiative capture on 3 H

Cited by 18 publications

References 63 publications

New results for radiative proton capture on 16O at astrophysical energies

New results for radiative proton capture on 16O at astrophysical energies

Reaction rate of p14N →15Oγ capture to all bound states in potential cluster model

The $^6$Li$(p, γ)^7$Be reaction rate in the light of the new LUNA data

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